The dataset is decimated to a sample rate of 2048 Hz. The PSD used in the likelihood is constructed using the median PSD estimation method described in Ref. [1]} with 8 s Hann-windowed segments (overlapped by 4 s) taken from GPS times (1167559424, 1167560448) for GW170104, (1180921982, 1180923006) for GW170608, (1185388936, 1185389960) for GW170729, (1186302007, 1186303031) for GW170809, (1186741349, 1186742373) for GW170814, (1187057815, 1187058839) for GW170818, and (1187528744, 1187529768) for GW170823. Prior to performing a Fourier transform of the data for PSD estimation, we remove the signal from the data used for PSD estimation by applying a gating window of width of the order of the signal length. This removes any bias introduced in the noise due to the presence of the signal. The PSD estimate is truncated to 4 s in the time-domain using the method described in Ref. [1]}.
For all seven events except GW170608, the likelihood is computed between a low-frequency cutoff of 20 Hz and the Nyquist frequency of 1024 Hz for all the detectors in the network. For GW170608, we use the same procedure in Ref. [3]} and compute the likelihood using a low-frequency cutoff of 20 Hz and the Nyquist frequency of 1024 Hz for the Livingston detector, and using frequencies between 30 Hz and 1024 Hz for the Hanford detector. During the observation of GW170608, the Hanford detector was undergoing a routine instrumental procedure to minimize angular noise coupling to the strain measurement. This introduced excess noise in the strain data from the Hanford detector at frequencies around \(\sim \) 19-23 Hz, but the strain data was shown to be stable above 30 Hz in Ref. [3]}.
